CHEMICAL ABUNDANCES FOR A-AND F-TYPE SUPERGIANT STARS

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CHEMICAL ABUNDANCES FOR A-AND F-TYPE SUPERGIANT STARS

R. E. Molina and H. Rivera

Laboratorio de Investigaci´on en F´ısica Aplicada y Computacional, Universidad Nacional Experimental del T´achira, Venezuela

Received May 9 2016; accepted July 11 2016

RESUMEN

Hemos efectuado un análisis detallado de las abundancias qu´ımicas de cuatro objetos supergigantes HD 45674, HD 180028, HD 194951 y HD 224893, usando espectros de alta resolución (R ≈ 42,000) tomados de la librer´ıa ELODIE. Se presentan los primeros resultados de las abundancias para HD 45674 y HD 224893, y se reafirman las abundancias para HD 180028 y HD 194951 calculadas por Luck. Los elementos alfa nos indican que todos los objetos estudiados pertenecen a la población del disco galáctico. Sus abundan-cias y su localización en el diagrama Hertzsprung-Russell parecen indicarnos que HD 45675, HD 194951 y HD 224893 evolutivamente se encuentran en la fase posterior al primer dragado (post-1DUP) y se mueven en la región del lazo rojo-azul (red-blue loop). HD 180028 muestra abundancias t´ıpicas de la Población I pero su estado evolutivo no puede ser definido satisfactoriamente.

ABSTRACT

We present the stellar parameters and elemental abundances of a set of A–F-type supergiant stars HD 45674, HD 180028, HD 194951 and HD 224893 us-ing high resolution (R≈42,000) spectra taken from ELODIE library. We present the first results of the abundance analysis for HD 45674 and HD 224893. We reaffirm the abundances for HD 180028 and HD 194951 studied previously by Luck. Alpha-elements indicate that the objects belong to the thin disc population. Their abun-dances and their location on the Hertzsprung-Russell diagram seem to indicate that HD 45675, HD 194951 and HD 224893 are in the post-first dredge-up (post-1DUP) phase, and that they are moving in the red-blue loop region. HD 180028, on the con-tary, shows typical abundances of Population I, but its evolutionary status cannot be satisfactorily defined.

Key Words:stars: abundances — stars: atmospheres — stars: evolution — super-giants

1. INTRODUCTION

The process of chemical evolution in the Galaxy can be understood from the study of its massive stars. These objects in their rapid evolution un-dergo changes through the process of nucleosynthesis and return their chemical elements to the interstel-lar medium by stelinterstel-lar winds and supernova events. The existence of massive young objects in the galac-tic plane is not surprising, since it is an area of star formation. These objects are visually luminous in galaxies and thus are suitable candidates for studies of stellar and chemical evolution (Luck et al. 1998;

Smiljanic et al. 2006; Venn et al. 2000, 2001, 2003; Kaufer et al. 2004).

Some of these massive objects have been classi-fied as supergiant stars with masses between 5 to 20M⊙, and A-and-F spectral types, which are mod-erately evolved. The chemical abundances of the light elements CNO have been crucial to discriminate their evolutionary states (Lyubimkov et al. 2011, Venn 1995a,1995b and references therein). When H is exhausted in massive stars the post-He core burn-ing phase can be affected in several ways.

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Stellar evolutionary models constructed for so-lar metallicities predict that massive supergiants (M≥10M⊙) are in the phase of helium core burning (Schaller et al. 1992; Stothers & Chin 1991). These objects have already left the main sequence and be-gun the ignition of He in the blue supergiant re-gion, but thermal instabilities cause in them a rapid expansion towards a red supergiant phase. In this phase, the A–F supergiants are able to resume ther-mal and radiative equilibrium through convection in the outer layers and shows an altered CNO abun-dance due to the first dredge-up (1DUP) event.

On the other hand, less massive A–F supergiants (M <10M⊙) have also initiated the He-core burning without visiting the red giant branch, they develop a fully convective intermediate zone, the envelope is able to establish thermal equilibrium and the stars stay in the blue supergiant phase. Under these condi-tions CNO abundances remain unchanged (Stothers & Chin 1976; 1991).

However, another scenario is possible for objects with intermediate masses (3<M<9M⊙) and it is called the blue loop. In this stage the star has even-tually developed a convective envelope and is ris-ing up the Hayashi line in the HRD. These objects have already reached the red supergiant stage but eventually evolve back into a blue supergiant phase (Walmswell et al. 2015). During the red supergiant phase, the convective zone mixes materials of the H-burning shell, which are subsequently released to the surface by the 1DUP event, causing changes in the observed CNO abundance patterns. The amount CNO-processed material in such objects allows us to discriminate between different types of supergiants.

The main goal of this work is a detailed study of chemical abundances for a set of four low-latitude A–F supergiants: HD 45674, HD 180028, HD 194951 and HD 224893, under the assumption of LTE, as well as the determination of their at-mospheric parameters from excitation and ioniza-tion equilibrium. For this purpose we employ high-resolution spectroscopy and a set of atmospheric mo-dels constructed with plane-parallel geometry, hy-drostatic equilibrium, local thermodynamic equilib-rium (LTE) and the ODFNEW _{opacity distribution} (Castelli & Kurucz 2004). It is expected that the abundances derived correspond to the typical abun-dances observed for supergiant stars in the galactic disc.

This paper is organized as follows: In§2 we de-scribe the sample selection. In §3 we present how the atmospheric parameters were estimated. We de-termine the chemical abundances for the three stars

Fig. 1. Representative spectra of the sample stars HD 45674, HD 180028, HD 194951 and HD 224893. The locations of lines of certain important elements have been indicated by dashed lines. This stars are arranged in de-creasing order the HD number.

in§4. An individual analysis of abundances for each stars is presented in §5. §6 is dedicated to discuss our results, and finally, §7 gives the conclusions of the paper.

2. OBSERVATIONS

2.1. Sample Selection

The stars for this analysis (HD 45674, HD 180028, HD 194951 and HD 224893) were selected because they are luminous objects of Classes I and II located in the galactic plane. The derived abundances are compared with the mean abundances obtained for a sample of G–K young supergiants of Population I taken from Luck (1977; 1978).

The stellar spectra taken for HD 45674, HD 180028, HD 194951 and HD 224893 are taken from the library ELODIE1 _{originally published by} Moultaka et al. (2001) and updated in its version 3.1 by Prugniel et al. (2007). The spectra were observed on July 06, 1999; on July 26, 2003; on December 18, 1999 and on July 07, 1999 respectively by means of the echelle spectrograph ELODIE placed in the 1.93m telescope located in the Haute-Provence Observatory (OHP). They cover the spectral region between 4000 and 6800 ˚A,and have a resolving power of R≈42,000. The signal-to-noise ratio (S/N) for

1

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BASIC PARAMETERS FOR THE SAMPLE

HD SpT α δ V B l b V_r π E(B−V) v sini

(h m s) (o′_”

) (mag) (mag) (o

) (o

) (km s−1₎ _(mas) _(mag) _{(km s}−1₎

45674 F1Ia 06 28 47 −00 34 20 6.56 7.30 210.85 −05.30 +18.4±0.9 1.31±0.51 0.382 · · · 180028 F6Ib 19 14 44 +06 02 54 6.96 7.73 040.97 −02.39 −5.1±0.7 -0.32±0.51 0.346 23.3 194951 F1II 20 27 07 +34 19 44 6.41 6.84 073.86 −02.34 −13.5±2.0 1.00±0.41 0.230 20 224893 A8II 00 01 37 +61 13 22 5.57 5.94 116.97 −01.07 −23.2±2.0 1.06±0.27 0.244 40

HD 45674, HD 180028, HD 194951 and HD 224893 is reported to be 83, 175, 82 and 145 respectively. This S/N per pixel has been derived for all spectra in the library at 5550 ˚A.

HD 45674, HD 180028 and HD 194951 are objects labeled as IRAS point sources, (IRAS 06262 - 0032, IRAS 19122 + 0557 and IRAS 20252 + 3410 respec-tively), although none of them display realiable in-frared excesses since their IRAS fluxes are of low quality (Q=1) at 25, 60 and 100 microns. A re-view of the spectral energy distributions (SED) from the available photometry contained in the VisieR database also indicates that flux data from other sources like WISE and AKARI for these three ob-jects do not indicate infrared excesses. Likewise, HD 224893 does not show evidence of dust around the central star. This last object was identified by Bidelman (1993) as a possible candidate to a post-AGB or normal A-and F-type supergiant star.

Figure 1 shows a representative range of 50 ˚A of the spectrum for the stars HD 45674, HD 180028, HD 194951 and HD 224893. The vertical dotted lines indicate the position of some absorption lines of el-ements such as YII, LaII, TiII, FeI y NiI. The basic parameters for the total sample are shown in Table 1. This table contains the HD number, the equatorial coordinates, the apparentV andB mag-nitude, the galactic coordinates, the radial velocity, the parallax, the color excess and the velocity of ro-tation. These values were taken from the SIMBAD astronomical database.2

3. ATMOSPHERIC PARAMETERS

In order to obtain the atmospheric parameters accurate measurements of the equivalent widths (Ew) of the Fe lines are necessary as well as mea-surements of atomic data (logg and χ (eV)). The atomic data for the FeI and FeII lines were taken from F¨uhr & Wiese (2006) and Mel´endez & Barbuy (2009). The Ew values were restricted to a range from 10 to 200 m˚A, and only non-blended lines were measured. To measure the Ew we used the task

2

http://simbad.u-strasbg.fr/simbad/

Fig. 2. Independence of FeI abundances from the low potential excitation and reduced equivalent widths in HD 45674 and HD 180028.

SPLOT _{of the} IRAF _{software with a Gaussian fit to}

the observed line profiles. The error in the measure-ments of Ew is about 8-10%.

The stellar atmospheric models for the abun-dance determinations were selected from the collec-tion of Castelli and Kurucz (2003). These models have been constructed with a plane-parallel geom-etry, hydrostatic equilibrium, local thermodynamic equilibrium (LTE) and theODFNEW_opacity distribu-tion.

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TABLE 2

ATMOSPHERIC PARAMETERS DERIVED IN THIS WORK AND THOSE OBTAINED FROM THE LITERATURE

HD Teff logg ξt [Fe/H] Ref.

(K) (km s−1

)

7346 1.95 +0.18 Prugniel & Soubiran (2001)

45674 7630 2.05 +0.16 Wu et al. (2011)

7488±₂₀₀ _2.00±_0.07 _+0.17±_0.01 _{Mean Value} 7500 2.0 4.0 +0.16 This Work (adopted) 6280 1.72 4.6 −_0.03 _{Gray et al. (2001b)} 6531 1.54 −_0.01 _{Prugniel & Soubiran (2001)} 6050 1.3 3.0 Andrievsky et al. (2002)

180028 6287 1.65 +0.14 Wu et al. (2011)

6307 1.9 4.0 +0.10 Kovtyukh et al. (2012)

6488 2.32 4.08 +0.26 Luck (2014)

6502 2.46 4.11 +0.39 Luck (2014)

6349±₁₇₁ _1.84±_0.42 _3.96±_0.59 _+0.14±_0.16 _{Mean Value} 6400 2.1 4.8 −_0.06 _{This Work (adopted)} 6950 2.02 −_0.09 _{Gray et al. (2001b)} 6350 1.0 2.8 Andrievsky et al. (2002)

194951 7392 Kovtyukh et al. (2007)

7268 Hohle et al. (2010)

6760 1.92 −_0.13 _{Lyubimkov et al. (2011)}

7019 2.22 3.93 +0.08 Luck (2014)

6977 2.21 3.87 +0.11 Luck (2014)

6959±₃₄₁ _1.87±_0.50 _3.53±_0.64 −_0.01±_0.12 _{Mean Value} 7000 1.8 4.7 −_0.15 _{This Work (adopted)} 224893 7340 1.96 3.9 −_0.24 _{Gray et al. (2001b)} 7500 2.0 4.5 −_0.26 _{This Work (adopted)}

rived by requiring that the FeI abundances be sim-ilar to those obtained for the FeII. To confirm the value of the gravity, the equilibrium condition can be extended to other elements with two ionization states like Ca, Ti, Cr, Ni. Finally the microturbu-lence velocity was determined by requiring that the abundances of FeI be independent of the reduced equivalent widths (log Ew/λ). Figure 2 shows that the abundances of FeI are independent of the low excitation potential and of the reduced equivalent widths for HD 45674 and HD 180028.

Table 2 lists the atmospheric parameters esti-mated by different authors from photometric and spectroscopic techniques and also the atmospheric parameters adopted for this work. For objects with more than one measure a mean value for their at-mospheric parameters was estimated. We note that our adopted atmospheric parameters match satisfac-torily these mean values.

3.1. Uncertainty in the Abundances

We calculated the effects on the chemical abun-dances of errors in the measured equivalent widths (8–10%), the defined model of atmospheric parame-ters (+250 K in Teff, +0.5 in logg and +0.5 km s−1 in ξt), and the atomic data (loggf andχ(eV)). Er-rors due to equivalent widths are random because they depend on several factors, such as the position of the continuum, the signal to noise ratio (S/N) and the spectral type of the star.

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SENSITIVITY OF ABUNDANCES TO THE INCERTAINTIES IN THE MODEL PARAMETERS FOR TWO RANGES OF TEMPERATURE SPANNING OUR SAMPLE STARS

HD 45674 HD 180028

(7500 K) (6400 K)

Species ∆Teff ∆logg ∆ξt ∆Ew σtot ∆Teff ∆logg ∆ξt ∆Ew σtot +250 K +0.5 +0.5 +10% +250 K +0.5 +0.5 +10%

CI −₀_.₁₄ ₀_.₀₀ ₊₀_.₀₁ −₀_.₀₁ ₀_.₁₄ ₊₀_.₀₇ −₀_.₁₁ −₀_.₀₁ ₀_.₀₀ ₀_.₁₃ NI −₀_.₀₂ −₀_.₀₆ ₀_.₀₀ −₀_.₀₁ ₀_.₀₆ · · · · OI +0.02 −₀_.₀₈ ₊₀_.₀₁ −₀_.₀₁ ₀_.₀₈ ₊₀_.₁₀ −₀_.₀₅ ₀_.₀₀ · · · ₀_.₁₁ NaI −₀_.₂₀ ₊₀_.₀₈ ₊₀_.₀₁ −₀_.₀₁ ₀_.₂₂ −₀_.₀₃ −₀_.₀₃ ₊₀_.₀₅ −₀_.₀₁ ₀_.₀₇ MgI −₀_.₂₂ ₊₀_.₀₈ ₊₀_.₀₈ −₀_.₀₁ ₀_.₂₅ −₀_.₁₄ −₀_.₀₄ ₊₀_.₀₄ ₀_.₀₀ ₀_.₁₅ SiI · · · −₀_.₀₃ −₀_.₀₃ ₊₀_.₀₁ ₀_.₀₀ ₀_.₀₄ SiII +0.02 −₀_.₀₈ ₊₀_.₁₆ −₀_.₀₂ ₀_.₁₈ ₊₀_.₁₃ −₀_.₁₅ ₊₀_.₀₇ −₀_.₀₁ ₀_.₂₁ SI −₀.17 +0.04 +0.02 −₀.01 0.18 +0.04 −₀.11 +0.02 −₀.01 0.12 CaI −₀.27 +0.10 +0.05 −₀.01 0.29 −₀.07 −₀.02 +0.04 −₀.01 0.08 CaII −₀.07 −₀.04 +0.03 0.00 0.09 · · · · ScII −₀_.₁₅ −₀_.₁₂ ₊₀_.₀₇ −₀_.₀₁ ₀_.₂₀ −₀_.₀₄ −₀_.₁₆ ₊₀_.₀₃ −₀_.₀₁ ₀_.₁₇ TiI −₀_.₂₈ ₊₀_.₀₅ ₀_.₀₀ −₀_.₀₂ ₀_.₂₉ −₀_.₁₄ −₀_.₀₄ ₊₀_.₀₁ −₀_.₀₁ ₀_.₁₅ TiII −₀_.₁₅ −₀_.₁₃ ₊₀_.₀₈ −₀_.₀₂ ₀_.₂₁ −₀_.₀₃ −₀_.₁₆ ₊₀_.₀₄ −₀_.₀₁ ₀_.₁₇ VII −₀_.₁₃ −₀_.₁₂ ₊₀_.₀₂ −₀_.₀₁ ₀_.₁₈ · · · · CrI −₀_.₂₇ ₊₀_.₀₆ ₊₀_.₀₃ −₀_.₀₁ ₀_.₂₈ −₀_.₁₂ −₀_.₀₄ ₊₀_.₀₃ −₀_.₀₁ ₀_.₁₃ CrII −₀_.₁₀ −₀_.₁₂ ₊₀_.₀₅ −₀_.₀₁ ₀_.₁₆ ₊₀_.₀₃ −₀_.₁₆ ₊₀_.₀₆ −₀_.₀₂ ₀_.₁₇ MnI −₀_.₂₄ ₊₀_.₀₇ ₊₀_.₀₂ −₀_.₀₁ ₀_.₂₅ −₀_.₀₈ −₀_.₀₄ ₊₀_.₀₄ −₀_.₀₁ ₀_.₁₀ FeI −₀_.₂₄ ₊₀_.₀₇ ₊₀_.₀₃ −₀_.₀₁ ₀_.₂₅ −₀_.₀₈ −₀_.₀₄ ₊₀_.₀₄ −₀_.₀₁ ₀_.₁₀ FeII −₀.10 −₀.12 +0.04 −₀.01 0.16 +0.02 −₀.15 +0.05 −₀.01 0.16 NiI −₀.22 +0.08 +0.01 0.00 0.23 −₀.08 −₀.04 +0.02 −₀.01 0.09 CuI · · · −₀_.₁₃ −₀_.₀₄ ₊₀_.₀₁ −₀_.₀₁ ₀_.₁₄ ZnI −₀_.₂₄ ₊₀_.₀₇ ₊₀_.₀₁ ₀_.₀₀ ₀_.₂₅ −₀_.₀₈ −₀_.₀₅ ₊₀_.₀₂ −₀_.₀₁ ₀_.₁₀ YII −₀_.₁₉ −₀_.₁₁ ₊₀_.₀₃ −₀_.₀₁ ₀_.₂₂ −₀_.₀₄ −₀_.₁₆ ₊₀_.₀₂ ₀_.₀₀ ₀_.₁₇ ZrII −₀_.₁₇ −₀_.₁₃ ₊₀_.₀₅ −₀_.₀₂ ₀_.₂₂ −₀_.₀₃ −₀_.₁₆ ₊₀_.₀₁ ₀_.₀₀ ₀_.₁₆ BaII −₀_.₃₀ ₀_.₀₀ ₊₀_.₀₅ −₀_.₀₁ ₀_.₃₀ −₀_.₁₀ −₀_.₁₀ ₊₀_.₀₇ · · · ₀_.₁₅ LaII · · · −₀_.₀₈ −₀_.₁₆ ₊₀_.₀₆ −₀_.₀₂ ₀_.₁₉ CeII −₀_.₂₄ −₀_.₀₈ ₊₀_.₀₁ −₀_.₀₁ ₀_.₂₅ −₀_.₀₈ −₀_.₁₅ ₊₀_.₀₁ ₀_.₀₀ ₀_.₁₇ NdII −₀_.₂₈ −₀_.₀₅ ₀_.₀₀ ₀_.₀₀ ₀_.₂₈ −₀_.₁₁ −₀_.₁₅ ₊₀_.₀₁ ₀_.₀₀ ₀_.₁₉ EuII · · · −₀.10 −₀.18 0.00 · · · ₀.20

may range from 10 to 25%. For neutron- capture el-ements the accuracy is in the 10 to 50% range. The sensitivity of the derived abundances to changes in the model atmosphere parameters is displayed in Ta-ble 3.

HD 45674 and HD 194951 have the same tem-perature, i.e., 7500 K. For these stars the spectra are much cleaner and the temperature is not large enough for the lines to develop strong wings making line strengths inaccurate. We can see that a vari-ation in effective temperature of 250 K generates a

greater uncertainty in all lines, particularly in neu-tral lines except C, N, O and ionized lines like Ba, Ce and Nd. On the contrary, we did not observe sig-nificant changes in the uncertainties due to changes in logg by 0.5, ξt by 0.5 km s−1 and Ew by 10 per cent. However, at a lower temperature (6400 K) the line strengths shows sensitivity only to changes both in Teff by 250 K, and in logg by 0.5.

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4. DETERMINATION OF THE ABUNDANCES

For the determination of chemical abundances we used the equivalent widths of 176, 116, 184 and 73 absorption lines identified in HD 45674, HD 180028, HD 194951 and HD 224893, respectively. We use the

task ABFIND _{of the} MOOG _{code (Sneden 1973). We}

employ the atmospheric models adopted in Table 2. The sources of the gf-values for different elements are those given by Sumangala Rao, Giridhar and Lambert (2012) (see Table 4 for further details).

Sumangala Rao, Giridhar and Lambert (2012) also studied the systematic differences caused when they used different sources for gf-values. The au-thors employed the solar spectrum from the Solar Flux Atlas (Kurucz et al. 1984) and found very few differences in the solar values for most of the ele-ments, i.e., between 0.04 to 0.09 dex.

The chemical abundances derived for HD 45674, HD 180028, HD 194951 and HD 224893 can be seen in Table 4. This table contains the chemical species present in the photosphere, the solar photospheric abundances as given by Asplund et al. (2005), as well as those calculated for each star and their un-certainty, the abundances relative to hydrogen, the number of identified lines and the abundances rel-ative to iron. The abundances of the elements in Table 4 are in a logarithmic scale with respect to hy-drogen, namely: logǫ(X) = log [N(X)/N(H)] + 12.0. The abundances of the elements relative to hydrogen and iron are expressed as [X/H] = logǫ(X)star - log

ǫ(X)sun and [X/Fe] = [X/H] - [Fe/H] respectively.

5. DISCUSSION OF THE INDIVIDUAL ABUNDANCES

5.1. HD 45674

The star HD 45674 has been classified as F1Ia. Bidelman (1993) includes this object as a possible candidate to a post-AGB or an A-and-F normal su-pergiant star. The atmospheric parameters were obtained from ionization equilibrium between the lines of FeI and FeII with values of Teff= 7500 K, logg= 2.0, χt= 4.0 and [Fe/H] = +0.16 dex respec-tively. The surface gravity for HD 45674 was con-firmed from the equilibrium ionization of other ele-ments such as Ca, Ti, Cr, from which ∆ = [XII/H]– [XI/H] is 0.08,−0.02 and−0.05 respectively. A com-pilation of the atmospheric parameters obtained by different authors is shown in Table 2.

With respect to the abundances of the light el-ements CNO, the carbon abundance was obtained from two lines (4769 ˚A and 5380 ˚A) their values being [C/H] =−0.20 and [C/Fe] =−0.36. Venn (1995b)

predicts a non-LTE correction of −0.25 in the C abundance for the supergiant HD 36673 (F0Ib) with an effective temperature of 7400 K. HD 45674 has an effective temperature of 7500 K; therefore no non-LTE correction was neccesary. A value of−0.25 dex led to an abundance of [C/Fe] =−0.69.

The N abundance for HD 45674 showed a moder-ate enrichement ([N/Fe] = +0.68). In fact, this abun-dance was obtained from theλ4151.4 ˚A line with an Ew of 10.1 m˚A. A non-LTE correction of−0.28 was derived by Venn (1995b) in the near IR region at 7400 K for this star, whis is of A9II type. The non-LTE correction for NI by Luck & Lambert (1985) indicated that at a temperature of 7500 K, an equiv-alent width of≈10 m˚A and logg= 2.0, the non-LTE correction is almost zero (see Figure 8). By contrast, for the blue region Przybilla & Butler (2001) found a non-LTE correction of−0.11 dex for NI(λ3830 ˚A) at a temperature of 9600 K and with a negatively increasing value toward the IR lines. Taking into consideration the above we can argue that the non-LTE correction should be small for this line.

We adopted a value of ≈ −0.08 dex for our line in the blue region. Our non-LTE values are [N/H] = +0.60 dex and [N/Fe] = +0.36 dex respec-tively. The observed deficiency of C and the moder-ate enhancement of N involves a conversion of initial carbon into N through the CN-cycle and products of the 1DUP being brought to the surface.

The O abundance is near solar ([O/Fe] = +0.03), and is obtained from the λ6156.0 ˚A and λ6156.8 ˚A lines. At this temperature a non-LTE correction of about −0.15 (taken from Takeda & Takada-Hidai 1998) would lead to abundances of [O/H] =−0.12 and [O/Fe] =−0.36 respectively. The C/O ratio of 0.32 indicates that HD 45674 is O-rich.

Iron-peak elements (Sc, V, Cr, Ni) show [X/Fe] abundances very similar to solar, and ranges from

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ELEMENTAL ABUNDANCES FOR HD 45674, HD 180028, HD 194951 AND HD 224893

HD 45674 HD 180028 HD 194951 HD 224893

Species logǫ⊙ [X/H] N [X/Fe] [X/H] N [X/Fe] [X/H] N [X/Fe] [X/H] N [X/Fe]

CI 8.39 −0.20±0.02 2 −0.36 −0.28±0.10 syn −0.22 −0.16±0.09 5 −0.01 −0.11±0.10 2 +0.15

NI 7.78 +0.68±0.06 1 +0.52 +0.89±0.06 1 +1.15

OI 8.66 +0.03±0.01 2 −0.13 +0.07±0.10 syn +0.13 −0.10±0.00 2 +0.05 +0.19±0.05 1 +0.45 NaI 6.17 +0.50±0.10 4 +0.34 +0.37±0.04 2 +0.43 +0.09±0.00 2 +0.24 +0.29±0.04 1 +0.55 MgI 7.53 +0.08±0.19 4 −0.08 +0.19±0.09 1 +0.25 −0.21±0.09 5 −0.06 −0.34±0.11 3 −0.08

SiI 7.51 +0.19±0.14 3 +0.25 +0.18±0.06 2 +0.33

SiII 7.51 +0.47±0.13 2 +0.31 +0.06±0.04 1 +0.12 −0.28±0.29 2 −0.02 SI 7.14 +0.41±0.10 5 +0.25 +0.38±0.09 3 +0.44 −0.03±0.10 syn +0.12

CaI 6.31 +0.24±0.11 8 +0.08 +0.07±0.13 5 +0.13 −0.13±0.17 10 +0.02 −0.29±0.03 4 −0.03

CaII 6.31 +0.16±0.15 2 0.00

ScII 3.05 +0.34±0.04 9 +0.18 +0.25±0.09 4 +0.31 −0.03±0.14 6 +0.12 +0.13±0.05 2 +0.39 TiI 4.90 +0.27±0.10 3 +0.11 +0.15±0.06 1 +0.21 −0.21±0.06 2 −0.06

TiII 4.90 +0.29±0.14 14 +0.13 +0.05±0.10 4 +0.11 −0.18±0.12 13 −0.03 −0.20±0.11 13 +0.06

VII 4.00 +0.22±0.02 1 +0.06 −0.24±0.02 1 +0.02

CrI 5.64 +0.13±0.08 3 −0.03 −0.11±0.10 2 −0.05 −0.34±0.13 5 −0.19 −0.25±0.12 2 +0.01 CrII 5.64 +0.18±0.12 7 +0.02 −0.11±0.13 3 −0.07 −0.25±0.11 11 −0.10 −0.40±0.09 4 +0.14 MnI 5.39 +0.14±0.01 3 −0.02 +0.11±0.08 4 +0.17 −0.21±0.18 5 −0.06 −0.21±0.03 1 +0.05

FeI 7.45 +0.12±0.10 60 −0.06±0.13 56 −0.17±0.11 72 −0.27±0.11 19 FeII 7.45 +0.20±0.08 10 −0.06±0.16 8 −0.12±0.11 20 −0.26±0.17 7 NiI 6.23 −0.06±0.12 8 −0.22 −0.09±0.06 4 −0.03 +0.10±0.11 6 +0.25

NiII 6.23 +0.01±0.04 1 +0.16

CuI 4.21 −0.26±0.04 1 −0.20

ZnI 4.60 −0.17±0.16 2 −0.33 −0.38±0.03 1 −0.32 −0.20±0.10 syn −0.05 −0.26±0.03 1 0.00 YII 2.21 +0.11±0.10 5 −0.05 +0.05±0.12 3 +0.11 −0.20±0.15 5 −0.05 −0.20±0.09 4 +0.06 ZrII 2.59 +0.61±0.13 3 +0.45 +0.10±0.04 1 +0.16 −0.12±0.19 2 +0.03

BaII 2.17 +0.35±0.07 1 +0.19 +0.23±0.10 syn +0.29 −0.11±0.07 1 +0.04 −0.34±0.10 2 −0.08

LaII 1.13 +0.29±0.05 1 +0.35

CeII 1.58 +0.33±0.14 3 +0.17 −0.08±0.16 3 −0.02

NdII 1.45 +0.22±0.05 1 +0.06 +0.13±0.09 2 +0.19 −0.11±0.17 2 +0.04

EuII 0.52 −0.12±0.10 syn −0.06

to +0.19 dex. Of other elements identified, like YII, BaII, CeIIand NdII, only ZrIIseems to be moder-ately enriched ([Zr/Fe] = +0.45).

5.2. HD 180028

HD 180028 was classified as a F6Ib and cataloged as anIRAS _{point source (IRAS 19122 + 0557). The} radial velocity was reported by different authors:

−6.0 km−1 _{(Wilson 1953),}₋_{6.0 km}−1 _{(Duflot et al.} 1995) and −5.1 km−1 _{(Gontcharov 2006) and does} not present variability. Its absorption lines appear slightly wide indicating that it rotates with a veloc-ity of 23.3 km−1 _{(De Medeiros et al. 2002).}

Their atmospheric parameters were obtained from ionization equilibrium between the lines of FeI

and FeII, with values of Teff= 6400 K, logg= 2.1,

χt= 4.8 and [Fe/H] =−0.06 dex respectively. The surface gravity for HD 180028 was confirmed from the equilibrium ionization of other elements such as Si, Ti, Cr, namely ∆ = [XII/H]–[XI/H] is 0.11,−0.10

and −0.00 respectively. The atmospheric parame-ters obtained by different authors and the adopted parameters are displayed in Table 2.

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O I

Fig. 3. Observed (filled squares) and synthetic (solid line) spectra of the OItriplet in the 6140–60 ˚A region. The synthetic spectra correspond from top to bottom to [O/H] = +0.37, +0.07 and−_{0.23 dex, respectively.}

[α/Fe] of +0.18±0.05 dex seems to indicate that this object belongs to the thin disk. Individually, Si, Ca and Ti present solar values while Mg shows a mod-erate enhancement, [Mg/Fe] = +0.25 dex. Sulfur is found be enriched, i.e., [S/Fe] = +0.44 dex. The s-elements show a solar trend except for Ba and La which are modestlly enhanced.

5.3. HD 194951

HD 194951 was classified as F-type by different authors: F2Iab by Stock et al.(1960), F3II by Bidel-man (1957) and F1II by Morgan (1972). The phys-ical parameters have been determined by various authors using photometric and spectroscopic tech-niques (see Table 2). The values we adopted can be seen in Table 3. The surface gravity of HD 194951 was confirmed from the equilibrium ionization of other elements, such as Ti, Cr, and Ni, from which ∆ = [XII/H]–[XI/H] is +0.05, +0.09 and −0.09 re-spectively. The chemical abundances of the elements identified are presented in Table 4.

The carbon abundance was determined from five lines (λ4769.9 ˚A, λ4775.8 ˚A, λ4932.0 ˚A, λ5380.3 ˚A andλ6014.8 ˚A). We obtained a [C/H] value of−0.16. At a temperature of 7000 K the non-LTE effects were present and a correction of−0.2 dex for carbon led to values of [C/H] =−0.36 and [C/Fe] =−0.26 re-spectively. For the O abundance a non-LTE cor-rection of −0.1 dex taken from Takeda & Takada-Hidai (1998) was estimated, and the abundances of

[O/H] =−0.20 and [O/Fe] = −0.10 are near to so-lar. These C and O abundance values are similar to those obtained by Luck (2014). The N line at

λ4151.4 ˚A found for HD 45674 and HD 224893 could not be measured. However, Lyubimkov et al. (2011) were able to study the N abundance for HD 194951 using high-resolution spectra and they found that N is enriched, with values of [N/H] = +0.60 and [N/Fe] = +0.73±0.18 respectively.

Our atmospheric model differs by 240 K and 0.12 in effective temperature and surface gravity relative to the model used by Lyumbikov et al., i.e., 6760 K and 1.92. In Table 3 we note that very few changes in the N abundance appear to be due to variations of 250 K and 0.5 in Teff and logg. This means that we can use this N abundance without being affected by the model. According to the authors the N en-richment is a general characteristic present in super-giant stars of A and F type that have experienced the first dredge-up (1DUP). The deficiency in C and the enrichment of N indicates that the CN-cycle has taken place and that processed material from the H-burning has been released on the surface of the star. The C/O = 0.46 ratio is practically solar, but it is an O-rich star.

The [α/Fe] ratio value of +0.06 is consistent for an object belonging to the thin disk population. The Si abundance exhibits a moderate enrichment, i.e., [Si/Fe] = +0.33. Other elements such as Sc, Cr, Mn and Zn show abundances [X/Fe] between−0.15 and +0.09, similar to those present in objects of the thin and thick disk. The Zn abundance was obtained from the synthesized line at λ4810.5 ˚A . [X/Fe] of the s-elements ranges from −0.09 to +0.01, that is, it is on average solar.

5.4. HD 224893

Gray et al. (2001b) determined atmospheric pa-rameters for this star (see Table 2) and it was clas-sified as a bright giant, A8II. Several authors stud-ied the radial velocity in different epochs, obtaining values (in km s−1_{) of} ₋_{22.4 (Adams 1915),} ₋_26.4 (Harper 1937),−23.2 (Wilson 1953),−21.9 (Bouigue et al. 1953),−27 (Fehrenbach et al. 1996) and−25.10 (Gontcharov 2006). These values show very little variation. Danziger & Faber (1972) report a rota-tion velocity of 40 km s−1_.

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respectively. From the LTE analysis we derived a value of [C/H] of −0.11 dex. By taking a non-LTE correction of −0.26 dex (Venn 1995b), both [C/H] and [C/Fe] reached values of −0.37 dex and

−0.19 dex respectively. The N abundances ob-tained fromλ4151.4 ˚A were [N/H] = +0.89 dex and [N/Fe] = +1.15 dex respectively. The equivalent width of this line was 15.8 m˚A. With a non-LTE cor-rection of−0.08 dex adopted at 7500K the new val-ues were [N/H] = +0.81 dex and [N/Fe] = +0.99 dex respectively. Like HD 45674, this star shows ev-idence of having undergone the CN-cycle and the 1DUP event.

The O abundance is derived from the line at 6158 ˚A and shows signs of overabundance ([O/Fe] = +0.45). However, a non-LTE correction of −0.15 dex at a temperature of 7500 K (from Takeda & Takada-Hidai 1998) leads to values of [O/H] = +0.35 dex and [O/Fe] = +0.53 dex respec-tively. These values indicate that the O abundance shows a moderate enrichment. The ratio C/O = 0.26 indicates that HD 224893 is O-rich and has a value similar to HD 45674.

The abundances [X/Fe] of the Fe-peak elements, such as V, Cr and Mn show solar values except Sc, which is moderately enriched by +0.39 dex. The alpha-elements ([α/Fe] =−0.02 dex); the Zn and the s-elements (Y and Ba) abundances resemble the solar values.

6. DISCUSSION

6.1. Atmospheric Parameters

The atmospheric parameters taken from the lit-erature and those adopted in this work are present in Table 2. We take a mean value of atmospheric parameters of those objects with more than two val-ues. We can note that our adopted values for the effective temperature, surface gravity, microturbu-lence velocity and metallicity are consistent (within the uncertainties) with the mean values derived by other authors.

6.2. Masses

We also estimated the masses of our sample stars. These can be obtained from their po-sition on the HR-diagram using theoretical evo-lutionary tracks. We employed the theoretical evolutionary tracks without rotation for masses of 5, 7 and 9M⊙, taken from Ekstr¨om et al. (2012) at solar metallicity (Z = 0.020). Lumi-nosities for HD 45674, HD 194951 and HD 224893

Fig. 4. Locations of HD 45675, HD 180028, HD 194951 and HD 224893 on the HR-diagram. The theoretical evolutionary tracks without rotation for masses of 5, 7 and 9M⊙ are taken from Ekstr¨om et al. (2012) with Z = 0.020.

were calculated using MV=V0+ 5−log(D), where

V0 is the intrinsic colour derived from expresion

V0=V −3.1E(B−V) and D is the distance esti-mated from parallaxes (van Leeuwen 2007).

For HD 180028, however, the absolute magnitude was derived from a mean value (MV=−3.38±0.16 mag) estimated by Kovtyukh et al. (2012). The bolometric corrections were taken from Masana et al. (2006) and we adopted a solar bolometric magnitude,

MBol= 4.73±0.01 (Gray 2005).

The color excesses for HD 180028, HD 194951 and HD 224893 were obtained using E(b−y) de-rived from Str¨omgren photometry by Gray et al. (2001b). We obtained E(B − V) from the rela-tion E(b−y) = 0.78E(B−V) (Fernie 1987). For HD 45674 the color excess was estimated from Schlafly’s map (Schlafly & Finkbeiner 2011) where the dust in the Galactic disc was modelled assuming a thin exponential disc with a scale-height of 125 pc. A correction to the color excess (B−V) was applied with the last assumption. The values are listed in the eleventh column of Table 1.

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and 0.21 (HD 224893). According to their position we could estimate that HD 180028 has a mass of between 5 and 7M⊙, HD 45674 and HD 194951 be-tween 7 and 7.5M⊙, and HD 224893 of about 9M⊙.

6.3. Evolutionary Status

CNO abundances are key to deduce the evolu-tionary status since their composition reflects the mixing process inside the stars. A summary is shown in Table 4. With respect to the light elements CNO, we note that the C abundances for HD 45674, HD 180028, HD 194951 and HD 224893 show defi-ciency with a non-LTE correction, i.e., they range from−0.04 to−0.69 dex.

Applying non-LTE corrections, HD 45674, HD 180028, HD 194951 and HD 224893 show values for the O abundance of −0.36, +0.02, −0.10 and +0.53, respectively. HD 224893, by contrast, has a moderate enhancement ([O/Fe] = +0.45) probably due to the CNO bi-cycle. In general, our oxygen values show the observed tendency in objects of the disc studied by Bensby et al. (2014); da Silva et al. (2015).

For the total sample we were able to iden-tify only one nitrogen line (λ4145.4 ˚A) for HD 45674 and HD 224893. The values with NLTE corrections are [N/Fe] = +0.36±0.11 dex and [N/Fe] = +0.99±0.14 dex, respectively. Both objects show signs of CN processed material that has been brought to the surface. Since we were unable to es-timate the abundance of nitrogen in HD 180028, we cannot argue about the efficiency of the CN-cycle. The N abundance in HD 194951 was previously studied by Lyubimkov et al. (2011), who found that nitrogen is enriched, i.e., [N/Fe] = +0.73±0.18 dex.

HD 45674, HD 194951 and HD 224893 show an enhancement of N abundance. These objects have shown a systematic deficiency of C and a systematic increase of N indicating the presence of CN-cycle ma-terial in the stellar surfaces. This enhancement of nitrogen was also reported by Venn (1995b), Venn & Przybilla (2003), Luck & Lambert (1985), Luck & Wepfer (1995) and Smiljanic et al. (2006) for super-giant and bright super-giant stars.

Three processes have been suggested to explain the surface nitrogen enhancement for massive stars. Each leads to the presence of CN-cycle material in stellar surfaces. In single stars these processes can be the severe mass loss, the rotationally induced mix-ing durmix-ing the MS phase and the dredge-up associ-ated with the deep convective envelope. According to Lyubimkov et al. (2011) the mass loss is unim-portant for B-type stars (progenitors of A–F

super-Fig. 5. Comparison of our abundances [X/H] with the mean abundances for a sample of G–K young supergiants taken from Luck (1977; 1978) and mean CNO abun-dances by Luck (2014). Symbols and color represent data from different sources. The color figure can be viewed online.

giants) with masses ranging between 4–15M⊙. By contrast, the other two processes might be found coupled, e.g., it is an observational fact that the mixing process during the 1DUP event might differ between rotating and non-rotating stars. In binary stars, on the contrary, this enhancement can be due to mass transfer from an evolved companion.

In order to verify whether HD 45674, HD 194951 and HD 224893 have already passed through the 1DUP event is necessary to know the [N/C] ratio. The post-1DUP prediction by Schaller et al. (1992) is approximately [N/C] = +0.60 dex for stars with masses between 2 and 15M⊙. On the other hand, Meynet & Maeder (2000) calculate rotating (with a initial velocity of 300 km s−1_{) and non-rotating} evolutionary models for masses between 9-120M⊙. These authors predict [N/C] = +0.72 dex without ro-tation and [N/C] = +1.15 dex with roro-tation after the 1DUP and during the blue loop phase for stars of 9M⊙. For more details see Figure 14 in Smiljanic et al. (2006).

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of −0.02 (in Teff) and−0.06 (in logg) respectively. These small differences do not affect the N abun-dance derived by Lyubimkov et al. (2011). Hence, it is possible to use the nitrogen abundance de-rived by Lyubimkov et al. (2011) with our C abun-dance. This value is [N/C] = +0.81±0.17 dex. For HD 45674 and HD 224893 we determined a [N/C] ra-tio of +0.88±0.09 dex and +1.00±0.13 dex respec-tively. We note also that these values indicate that both stars show signs of an efficient mixing pro-cess. The mean [N/C] ratio for the sample stars is [N/C] = +0.90±0.13 dex.

In short, our results for single and mean [N/C] ratios are larger than the values obtained by Schaller et al. (1992) by a factor between 0.3-0.4 dex and are slightly above those of the non-rotating model of by Meynet & Maeder (2000), i.e., between +0.72 dex (non-rotating model) and +1.15 dex (ro-tating model). Our mean value +0.90±0.10 dex would be in agreement with the results for non-rotating stars with masses of 9M⊙. Therefore, we may conclude that within the range of masses of our objects (5–9M⊙) and for their [N/C] ratios, HD 45674, HD 194951 and HD 224893 have already experienced the 1DUP event and are in post-1DUP phase. Evolutionarily, the post-1DUP objects can be located only inside the red-blue loop area. Claret (2004) suggests that extensive red-blue loops occur for stars with masses from 6 to 13M⊙, although this extension is still a matter of controversy (see§6 and Figure 12 in Lyubimkov et al. 2011).

On the other hand, if we consider the ef-fective temperature and luminosities to be right, HD 45674, HD 194951 and HD 224893 appear to be located within the extended red-blue region with

M = 7−9M⊙ on the HR-diagram. However, the uncertainties cause an appreciable change in the lu-minosity so that their evolutionary status is unreli-able. With regard to HD 180028, assuming a mass of 5M⊙, its probable evolutionary status would place it in the red-blue loop region (post-1DUP phase). On the contrary, if we assume a mass of 7M⊙ it would to be located on the Hertzsprung gap region and moving for the first time towards the red gi-ant/supergiant phase (post-MS phase).

6.4. Sodium

In our sample we found a moderate enrichment of Na abundances, i.e., [Na/Fe] of +0.34, +0.43, +0.24 and +0.55 for HD 45675, HD 180028, HD 194951 and HD 224893, respectively. It is believed that the sodium enrichment is related to the first dredge-up

this assumption is still debated. The predictions made by the models (see Fig. 8 in Karakas & Lat-tanzio 2014) indicate that sodium does not show a significant enrichment in low-mass stars (M≤2M⊙) from the first dregde-up or by extra-mixing process to solar metallicity (Charbonnel & Lagarde 2010). Even forM >2M⊙ this enrichment does not exceed 0.3 dex.

A non-LTE correction of about of−0.10 dex to Na was taken from Lind et al. (2011) and results in values of [Na/Fe] of +0.16, +0.22, +0.24 and +0.37 dex respectively. We note that our obser-vational results (within their uncertainties) are in agreement with the [Na/Fe] predicted by El Eid & Champagne (1995) for intermediate mass stars (≈0.2-0.3 dex).

6.5. Heavier Elements

The tendency shown by the alpha-elements of our objects is similar to that observed in the thin disk population, i.e., [α/Fe] ranges from −0.02 to 0.18 dex. The sulfur abundance was estimated syn-thesizing the spectral region at (6743–6757 ˚A). We obtained a [S/Fe] of +0.25 for HD 45675 and +0.12 for HD 194951, showing a tendency similar to that observed for α-elements in the disc for metallic-ity near to solar value (Caffau et al. 2005). By contrast, S for HD 180028 is overabundant, i.e., [S/Fe] = +0.44 dex. Iron-peak and neutron-capture elements in all sample stars show [X/Fe] abundances similar to the solar value. HD 45674 and HD 180028 show a modest enrichment of ZrII and LaII of +0.45 dex and +0.32 dex, respectively.

6.6. Comparison With Other Supergiants

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7. CONCLUSIONS

We performed a detailed analysis of the photo-spheric abundances for a sample of four A–F type supergiant stars of intermediate mass (≈5–9M⊙) us-ing high-resolution spectra. We determined atmo-spheric parameters, masses and abundances using spectral synthesis and equivalent widths. Three stars (HD 45674, HD 194951 and HD 224893), for which we were able to determine both carbon and nitro-gen, show signs of internal mixing. A mean [N/C] ratio of +0.90±0.13 dex was found; this value is in agreement with the preditions of non-rotating mo-dels by Meynet & Maeder (2000), which predict [N/C] =+0.72 dex. A surface nitrogen enhancement was observed in these stars and it can only be a re-sult of deep mixing during the 1DUP. The sample of three stars shows very little variability in radial velocities, and hence binarity can be discarded.

According to the abundance analysis we can con-clude that HD 45674, HD 194951 and HD 224893 have abundance values typical for supergiants of the thin disc population that have reached the post-first dregde-up (post-1DUP) phase. These objects are lo-cated in the red-blue loop region. HD 180028, on the contrary, shows abundances typical of Population I, but its evolutionary status could not be satisfactorily determined.

This work has made extensive use of ELODIE, SIMBAD and ADS-NASA databases for which we are thankful. The authors thank an anonymous ref-eree for fruitful comments and suggestions that im-proved this work.

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